The distribution of the braking
force will be calculated
if the magnetic field structure inside the star is given, and
thereafter one can discuss the angular momentum
transfer inside the star.
The spin-down evolution including the glitches and any other kinds of timing
noise was discussed with the two-component, crust-superfluid, models
[1]}, [2]}, [3]}, where
the torque distribution inside the star was not taken into account.
Our present study demonstrates that
the braking torque distribution
for a given magnetic field can be calculated and hence
a more detailed modelling of the spin-down history than ever conducted is possible.
Furthermore, the resultant models can
be compared with
observations of timing irregularities of pulsars to
gain deeper insight about
the magnetic structure inside the neutron star.
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